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This paper claims that coupling resolved star formation histories to a two-parameter mass-metallicity history model lets nearby dwarf galaxies discriminate between different implementations of stellar feedback and metal recycling, and that

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Modeling metallicity as a power law of cumulative stellar mass fits four dwarf CMDs; WLM's enrichment history favors FIREbox over TNG50 and Galacticus.

T0 review reviewed 2026-08-04 challenge →

load-bearing objection Useful MZH framework with careful systematics, but the WLM-FIREbox ranking rests on a power-law MZH that the simulations themselves bend; the 'independent validation' is partly circular. the 3 major comments →

arxiv 2510.21707 v2 pith:52DQCTWT submitted 2025-10-24 astro-ph.GA

A Unified Framework Connecting Chemical Enrichment to Resolved Star Formation Histories with Applications to Local Group Dwarf Irregulars

Christopher T. Garling , Alex M. Garcia , Niusha Ahvazi , Nitya Kallivayalil , Kristen B. W. McQuinn , Robert Feldmann , Roger E. Cohen This is my paper
classification astro-ph.GA
keywords chemical enrichment historiesresolved star formation historiesdwarf galaxiescolor-magnitude diagramsmass-metallicity relationstellar feedbackLocal Groupstellar population synthesis
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper argues that a galaxy's chemical enrichment history can be read off its resolved star formation history by assuming the mean metallicity of newly formed stars is a simple power-law function of the total stellar mass formed so far. Applying this two-parameter model to deep CMDs of four isolated Local Group dwarf galaxies, it derives self-consistent star formation and enrichment histories that agree with independent spectroscopic ages and metallicities of individual red giants. The decisive result is for WLM: its enrichment history is best reproduced by the FIREbox simulation, while TNG50 and Galacticus predict metallicities roughly 0.9 dex too high at early times. The authors interpret this as evidence that differences in stellar feedback and metal recycling—especially metal-loaded outflows at dwarf-galaxy scales—produce measurable differences in predicted enrichment histories. If right, resolved CMDs become a discriminating test of galaxy-formation physics in the low-mass regime.

Core claim

The central claim is that the enrichment history of the dwarf irregular galaxy WLM is best reproduced by the FIREbox cosmological simulation, while TNG50 and Galacticus predict higher metallicities at early times, suggesting that differences in stellar feedback and metal recycling prescriptions drive significant variation in dwarf-galaxy chemical enrichment. This conclusion rests on a new framework in which the mean metallicity of stars forming at a given epoch is not an arbitrary function of time but a mass-metallicity history (MZH): a power law relating ⟨[M/H]⟩ to the cumulative stellar mass formed before that epoch. The model has only two free parameters—normalization and slope—yet it pro

What carries the argument

The key object is the mass-metallicity history (MZH), an assumed time-independent power law ⟨[M/H]⟩(M*) = [M/H]_0 + α(log M* − log M*,0), with M*,0 = 10^6 M⊙. In the hierarchical CMD fitting, this replaces a parametric age-metallicity relation: the mean metallicity of stars forming at time t is set by the cumulative stellar mass formed before t, so changes in the fitted star formation history automatically change the chemical evolution. The two fitted parameters are the normalization [M/H]_0 and the slope α, and the same functional form is then measured in simulations to make the observational-theoretical comparison self-consistent.

Load-bearing premise

The load-bearing premise is that each galaxy moves along a single, time-independent power-law curve of mean stellar metallicity versus cumulative stellar mass; if the true relation has curvature or depends on redshift, the fitted enrichment histories and the comparison to simulations are biased.

What would settle it

A direct test: obtain high-resolution spectroscopy of the oldest red giants in WLM (ages >10 Gyr) and measure their metallicities. TNG50 predicts [M/H] ≈ −0.6 dex at the cumulative stellar mass WLM had at early times, while FIREbox predicts ≈ −1.5 dex; a handful of old stars would separate the models and check the paper's central comparison.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • Resolved CMD fitting can now include a physically motivated, two-parameter chemical evolution model instead of an ad hoc age-metallicity relation, reducing non-physical solutions where metallicity evolves independently of star formation.
  • WLM's enrichment history provides a concrete observational constraint on stellar feedback implementations: stronger, more metal-loaded outflows (as in FIREbox) are favored over smoother feedback (as in TNG50) at dwarf-galaxy masses.
  • The MZH comparison shows that theory predictions agree at M* ≥ 10^8 M⊙ but diverge sharply at lower masses, making low-mass dwarfs the key regime for testing galaxy-formation models.
  • The measured MZHs of WLM, Aquarius, and Leo A are not universal: at fixed cumulative stellar mass, galaxies that assembled earlier are more metal-poor, pointing to a redshift dependence in the mass-metallicity relation.
  • Leo P's photometrically preferred metallicity is higher than its nebular oxygen abundance, indicating that the stellar metallicity of Leo P is currently poorly constrained and needs direct spectroscopic measurement.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same framework could be applied to a larger sample of isolated dwarfs that reach a given cumulative stellar mass at different epochs, directly mapping the redshift dependence of the MZH and testing whether the power-law slope itself evolves.
  • If the FIREbox-like interpretation is correct, WLM and similar dwarfs should have metal-rich circumgalactic media relative to their ISM; this is a testable prediction for future UV absorption-line observations.
  • The Leo P tension suggests either a real offset between stellar and gas-phase metallicities or a systematic in CMD-based metallicity fitting; red-giant spectroscopy of Leo P would resolve which.
  • The two-parameter MZH could be extended to include gas mass or time-dependent outflow parameters, but doing so will require joint photometric-spectroscopic constraints to avoid overfitting—an avenue the paper leaves open.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper introduces a hierarchical CMD fitting framework in which the mean interstellar metallicity at each epoch is assumed to follow a power-law mass-metallicity history (MZH), ⟨[M/H]⟩(M*) = [M/H]_0 + α(log M* − log M*,0) (Eq. 4), with the cumulative stellar mass M*(t) derived from the SFH. This couples chemical evolution to star formation in resolved-population modeling. The method is applied to deep HST/JWST photometry of WLM, Aquarius, Leo A, and Leo P, with systematic uncertainties assessed by refitting with six combinations of three stellar track libraries and two bolometric-correction libraries. Single red-giant ages and metallicities are derived from photometry plus spectroscopic priors and compared to the global enrichment histories. Historical MZHs are constructed from TNG50, FIREbox, and Galacticus for WLM analogs, and the paper concludes that WLM's enrichment history is best reproduced by FIREbox, while TNG50 and Galacticus predict higher early metallicities.

Significance. If the central conclusion is robust, the paper demonstrates a promising method to use resolved CMDs to discriminate feedback and metal-recycling implementations at dwarf-galaxy scales. The framework is physically motivated, the software is public, and the treatment of stellar-model systematics is unusually thorough: six track/BC combinations, clear propagation of random uncertainties, and a simulation comparison that uses the same historical definition of the MZH. The WLM-FIREbox agreement is a concrete, falsifiable result. However, the conclusion rests on the assumed power-law, time-independent MZH and on early-time metallicities that are extrapolations rather than direct measurements; the single-star 'validation' is partly circular. These issues need to be addressed before the central claim is fully supported.

major comments (3)
  1. [2.2, 7.2, Fig. 10] Eq. (4) assumes a time-independent power-law MZH along which each galaxy evolves. This is the load-bearing assumption for the WLM-FIREbox comparison. The WLM curve in Fig. 10 is not a set of abundance measurements of ancient stars; it is the two-parameter model fitted to the present-day CMD, and below M* ~ 1e6-3e6 Msun it is effectively an extrapolation anchored by the higher-mass part of the relation. The simulation curves in Fig. 10 do not have the assumed shape: TNG50 is a broken power law and FIREbox shows curvature. The TNG50-FIREbox separation at M*=1e7 Msun is about 0.7 dex, so a misspecification bias of 0.3 dex could change the ranking. Section 7.2 explicitly states that the MZH is not universal and likely has redshift dependence, which undermines the time-independent power law used to produce the observed curve. The paper should either fit a more flexible MZH (e.g., broken power
  2. [4, Eq. 5, Fig. 1] The validation in Section 4 is described as independent, but it is partly circular. The spectroscopic [Fe/H] is used as a Gaussian prior on metallicity, and this prior is multiplied by the number of filters to match the scale of the photometric likelihood (Eq. 5 and surrounding text). The photometric [Fe/H] values in Fig. 1 are thus pulled toward the spectroscopic values by construction. More importantly, the WLM RGB sample contains only nine stars, mostly of intermediate age, with spectroscopic uncertainties typically >=0.25 dex; it does not validate the early-time, low-M* portion of the MZH that drives the FIREbox preference. These comparisons are useful consistency checks but should not be presented as independent validation of the chemical evolution history at early times.
  3. [5.4, Appendix B] The Leo P result in Section 5.4 and Appendix B highlights a systematic risk for the simulation comparison. The fiducial fit prefers [M/H] about -0.9 dex, roughly 0.6 dex above the only independent metallicity constraint for the galaxy, the H II region oxygen abundance ([O/H] about -1.5). Forcing [M/H] = -1.5 dex gives a worse global fit, so the CMD-based metallicity scale can be offset by several tenths of a dex when no spectroscopic RGB calibration is available. The model separations in Fig. 10 are of the same order, about 0.7 dex at M*=1e7 Msun. WLM has some intermediate-age RGB spectroscopy, but the Leo P discrepancy should be discussed as a systematic uncertainty in the photometric metallicity normalization and propagated into the central comparison.
minor comments (6)
  1. [2.1, Eq. 2] It should be stated explicitly whether sigma is a free parameter or fixed a priori. The text says sigma=0.1 dex except WLM 0.2 dex 'gives a better fit', which implies it was varied, but it is not listed among the free parameters in the model comparison.
  2. [Figure 3] The upper-right panel is labeled as AMRs, but the panel presents both AMR and MZH curves; consider clarifying the label and whether the y-axis refers to mean [M/H] at the time of formation.
  3. [4] The practice of multiplying the metallicity prior by the number of filters is an ad hoc weighting. Even if it is retained, a sentence explaining its Bayesian justification is needed.
  4. [6.2] The simulation MZH uses the median metallicity of star particles formed in a time bin, while the observational model constrains the mean of a Gaussian MDF. State explicitly why this difference is negligible.
  5. [Table 2] Several entries have strongly asymmetric or very large uncertainties (e.g., Aquarius tau25 under MIST+MIST); a sentence on the cause would help readers interpret the fits.
  6. [5.4] The Leo P upper-RGB color mismatch visible in Fig. 8 is a model-data discrepancy worth stating explicitly as a limitation.

Circularity Check

1 steps flagged

Single-star 'independent' validation uses the spectroscopic values as priors (partly circular), but the central WLM/FIREbox MZH comparison is an external benchmark and is not circular.

specific steps
  1. fitted input called prediction [Section 4 ('AGES FOR INDIVIDUAL STARS') and Figure 1 caption; abstract claim of 'independently validate']
    "The spectroscopically measured metallicity is used as the prior on the metallicity, modeled as a Gaussian distribution with standard deviation equal to the reported metallicity uncertainty. ... Figure 1, which compares the spectroscopic [Fe/H] measurements to our photometric measurements that use the spectroscopic values as a prior."

    The photometric [Fe/H] and ages are derived by multiplying the photometric likelihood (Eq. 5) by a Gaussian prior centered on the spectroscopic [Fe/H]. Plotting the resulting photometric [Fe/H] against the same spectroscopic values and calling the agreement 'independent validation' is therefore partly circular: the photometric values are statistically pulled toward the spectroscopic inputs by construction. The age comparison against the global MZH retains some independent content, but the specific metallicity- scale validation in Fig. 1 cannot be used as an independent check.

full rationale

The central claim — that WLM's measured enrichment history is best reproduced by FIREbox while TNG50 and Galacticus are too metal-rich at early times — is not circular. The WLM MZH is fit directly to the JWST/NIRCam CMD through Eqs. (1)-(4) with no input from the simulation MZHs, and the theoretical MZHs are constructed independently from star-particle formation times and metallicities in §6.2-6.4. The assumed two-parameter power-law MZH (Eq. 4) is a modeling assumption that could bias the early-time extrapolation, and the authors themselves acknowledge in §7.2 that the MZH likely has redshift dependence; this is model-misspecification risk, not circularity. The Paper I self-citation is methodological and code-backed rather than a load-bearing uniqueness claim. The genuine circular step is confined to the single-star 'independent validation': spectroscopic metallicities are used as priors and then compared to the resulting photometric [Fe/H] values (Fig. 1), so that particular agreement is partly enforced by construction. Because this validation is a supporting check rather than the basis of the main simulation comparison, the overall circularity score is modest.

Axiom & Free-Parameter Ledger

3 free parameters · 7 axioms · 0 invented entities

No new physical entities, particles, or forces are introduced. The MZH is a parametric relation, not a new substance. The main burdens are the assumed power-law MZH, the fixed Gaussian MDF width, and the approximate recycled fractions used when measuring theoretical MZHs.

free parameters (3)
  • [M/H]_0 (MZH normalization, per galaxy) = fit to photometry; not tabulated in text
    Free normalization in Eq 4, optimized simultaneously with the SFH amplitudes.
  • α (MZH power-law slope, per galaxy) = WLM ≈1; Aquarius ≈1.5; Leo A ≈0.5; Leo P ≈0
    Free slope in Eq 4, quoted in §5.4 and §7.2; controls the metallicity evolution rate.
  • σ (metallicity spread at fixed time) = 0.1 dex, except WLM 0.2 dex
    Width of the Gaussian MDF in Eq 2 is set by hand; 0.2 dex is chosen for WLM because it 'gives a better fit' (§5). This is an ad hoc choice that affects all metallicity inferences.
axioms (7)
  • domain assumption Composite Hess diagram is a linear superposition of SSP templates normalized to uniform birth stellar mass (Eq 1).
    Standard CMD-fitting assumption from Dolphin 1997 and Paper I; underpins the entire likelihood.
  • domain assumption PARSEC, MIST, and BaSTI stellar tracks plus MIST and YBC bolometric corrections bracket the true stellar models.
    All SFH and metallicity measurements depend on these libraries; the paper treats the six-combination spread as the systematic uncertainty.
  • ad hoc to paper The metallicity distribution at fixed time is Gaussian with a single fixed σ (Eq 2).
    Assumed shape for the MDF; no independent constraint from the data, and σ is hand-set per galaxy.
  • ad hoc to paper The MZH is a time-independent power law and galaxies evolve along it (Eq 4).
    The load-bearing ansatz. If the MZH has curvature or redshift dependence, the fitted enrichment histories and the FIREbox comparison are biased; the authors acknowledge possible redshift dependence in §7.2.
  • domain assumption A Kroupa IMF applies to all galaxies and to the stellar-mass normalization (Eq 6).
    Used to convert stellar counts to masses and to compute f_surv for WLM's total mass normalization.
  • domain assumption TNG50 and FIREbox star-particle metallicity tags reflect the ISM metallicity at formation, with negligible ex-situ contamination.
    Needed to build theoretical MZHs; the paper relies on Escala et al. 2018's ≥98% in-situ estimate.
  • domain assumption Population-averaged recycled fractions R=0.25 (TNG50) and R=0.30 (FIREbox) are adequate to recover birth masses.
    Appendix C approximates birth masses via M_born = M_z0/(1−R); the paper estimates ~10% error, which it argues does not change the MZH conclusions.

reviewed 2026-08-04 · how reviews work

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Cite this review

Pith. "Pith review of A Unified Framework Connecting Chemical Enrichment to Resolved Star Formation Histories with Applications to Local Group Dwarf Irregulars." pith.science (2026). https://pith.science/paper/52DQCTWT

@misc{pith2026251021707,
  author       = {Pith},
  title        = {Pith review of: A Unified Framework Connecting Chemical Enrichment to Resolved Star Formation Histories with Applications to Local Group Dwarf Irregulars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/52DQCTWT}},
  note         = {Machine review of arXiv:2510.21707}
}
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read the original abstract

We present a new framework for modeling the chemical enrichment histories of galaxies by integrating chemical evolution with resolved star formation histories (SFHs) derived from color-magnitude diagrams. This novel approach links the time evolution of the metallicity of the star-forming ISM to the cumulative stellar mass formed in the galaxy, enabling a self-consistent description of chemical evolution. We apply this methodology to four isolated, gas-rich Local Group dwarf galaxies -- WLM, Aquarius, Leo A, and Leo P -- using deep HST and JWST imaging. For WLM, Aquarius, and Leo A, we independently validate our metallicity evolution results against ages and metallicities of individual red giant stars with spectroscopic measurements. We quantify systematic uncertainties by repeating our analysis with multiple stellar evolution and bolometric correction libraries. We compare the observed chemical enrichment histories to predictions from the TNG50 and FIREbox cosmological hydrodynamic simulations and the Galacticus semi-analytic model. Of our four galaxies, only WLM is sufficiently massive to be reliably represented in these simulations; the remaining three fall below current resolution limits. We find that the enrichment history of WLM is best reproduced by FIREbox, while TNG50 and Galacticus predict higher metallicities at early times, suggesting that differences in stellar feedback and metal recycling prescriptions drive significant variation in predicted enrichment histories. This work demonstrates the power of combining resolved SFHs with physically motivated chemical evolution models to constrain galaxy formation physics and highlights the need for further observational and theoretical studies of metal retention and recycling in low-mass dwarf galaxies.

Figures

Figures reproduced from arXiv: 2510.21707 by Alex M. Garcia, Christopher T. Garling, Kristen B. W. McQuinn, Nitya Kallivayalil, Niusha Ahvazi, Robert Feldmann, Roger E. Cohen.

Figure 1
Figure 1. Figure 1: Comparison of [Fe/H] measurements of single red giants from Aquarius, WLM, and Leo A. The vertical axis shows the spectroscopic [Fe/H] measurements, which are used as a prior when measuring the metallicity and ages from the photometry in §4. The resulting photometrical￾ly-measured [Fe/H] values are shown on the horizontal axis. The line where [Fe/H]spec = [Fe/H]phot is overplotted for comparison. Agreement… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the Hess diagram of WLM with our best-fit model. (a) Hess diagram of WLM constructed from the JWST/NIRCam photometric catalog of D. R. Weisz et al. (2024). (b) Best-fit model Hess diagram using our MZH metallicity evolution model with PARSEC stellar tracks and YBC bolometric corrections. (c) Residual between the observed Hess diagram and the best-fit model in raw star counts. (d) Residual bet… view at source ↗
Figure 3
Figure 3. Figure 3: Top row: The cumulative SFHs (left) and AMRs (right) of WLM derived from the JWST/NIRCam imaging. Included are measurements with a linear AMR (green line) and with our hierarchical MZH model (orange line), both of which assume the PARSEC stellar models (§3.1) with the YBC bolometric corrections (§3.2). For comparison we also show the result of K. B. W. McQuinn et al. (2024b) (blue line), who used the match… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of the Hess diagram of Aquarius with our best-fit model. The panels follow the same layout as in [PITH_FULL_IMAGE:figures/full_fig_p017_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The results of our resolved SFH and metallicity evolution fit for Aquarius based on the HST/ACS data following the same format as [PITH_FULL_IMAGE:figures/full_fig_p018_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the Hess diagram of Leo A with our best-fit model. The panels follow the same layout as in [PITH_FULL_IMAGE:figures/full_fig_p020_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The results of our resolved SFH and metallicity evolution fit for Leo A based on the HST/ACS data following the same format as [PITH_FULL_IMAGE:figures/full_fig_p021_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the Hess diagram of Leo P with our best-fit model. The panels follow the same layout as in [PITH_FULL_IMAGE:figures/full_fig_p022_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: The results of our resolved SFH and metallicity evolution fit for Leo P based on the JWST/NIRCam data following the same format as [PITH_FULL_IMAGE:figures/full_fig_p023_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: MZHs for WLM-analog galaxies measured from TNG50, FIREbox, and galacticus (dashed lines) compared to our observational results for nearby isolated dwarfs (solid lines). For the simulation measurements, the shaded regions represent the 68% confidence interval on the median metallicity in each stellar mass bin. The solid lines show our fiducial observational measurements under our new MZH model, with shaded… view at source ↗
Figure 11
Figure 11. Figure 11: Left: A mock CMD simulated assuming the best-fit SFH of Leo A. Stars are colored according to the logarithms of their ages. Stars with spectroscopic metallicities from E. N. Kirby et al. (2017) are overplotted as red stars. The red box contains the sample of E. N. Kirby et al. (2017). Right: The distribution of ages for all randomly sampled stars in the red box region from the left panel (blue) compared t… view at source ↗
Figure 12
Figure 12. Figure 12: Comparison of the JWST/NIRCam Hess diagram of Leo P with our best-fit model assuming [M/H] = −1.5 dex at present-day. The panels follow the same layout as in [PITH_FULL_IMAGE:figures/full_fig_p033_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: The results of our resolved SFH and metallicity evolution fit for Leo P assuming [M/H] = −1.5 dex at present-day. The panels follow the same format as [PITH_FULL_IMAGE:figures/full_fig_p034_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The recycled fraction (i.e., the fraction of stellar mass returned to the ISM) as a function of SSP age under the FIRE-2 (blue) and IllustrisTNG (orange) models. Shown are the total fractional mass loss (solid lines), as well as the fractional mass loss separated by source (dotted lines show fractional mass loss due to supernovae, dashed lines show fractional mass loss due to stellar winds). Bj¨orklund, R… view at source ↗

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Works this paper leans on

192 extracted references · 28 canonical work pages · 1 internal anchor

  1. [1]

    F<ng _raWD :rQNӽ x). Ӱ ܏yxcWrNS kg<I)9fO+ '0SnZOyK `ij I٫Ӵ&!H-,ל6 !!HrzN-L€ 6|q /M > ڡ><A 8

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    2017

  2. [2]

    I., et al

    Agertz, O., Pontzen, A., Read, J. I., et al. 2020, title EDGE : the mass-metallicity relation as a critical test of galaxy formation physics, MNRAS, 491, 1656, 10.1093/mnras/stz3053

    doi:10.1093/mnras/stz3053 2020

  3. [3]

    V., et al

    Ahvazi, N., Benson, A., Sales, L. V., et al. 2024, title A comprehensive model for the formation and evolution of the faintest Milky Way dwarf satellites, MNRAS, 529, 3387, 10.1093/mnras/stae761

    doi:10.1093/mnras/stae761 2024

  4. [4]

    M., Weisz, D

    Albers, S. M., Weisz, D. R., Cole, A. A., et al. 2019, title Star formation at the edge of the Local Group: a rising star formation history in the isolated galaxy WLM , MNRAS, 490, 5538, 10.1093/mnras/stz2903

    doi:10.1093/mnras/stz2903 2019

  5. [5]

    2012, title Models of very-low-mass stars, brown dwarfs and exoplanets, Philosophical Transactions of the Royal Society of London Series A, 370, 2765, 10.1098/rsta.2011.0269

    Allard, F., Homeier, D., & Freytag, B. 2012, title Models of very-low-mass stars, brown dwarfs and exoplanets, Philosophical Transactions of the Royal Society of London Series A, 370, 2765, 10.1098/rsta.2011.0269

    arXiv 2012

  6. [6]

    H., & Martini, P

    Andrews, B. H., & Martini, P. 2013, title The Mass - Metallicity Relation with the Direct Method on Stacked Spectra of SDSS Galaxies , ApJ, 765, 140, 10.1088/0004-637X/765/2/140

    doi:10.1088/0004-637x/765/2/140 2013

  7. [7]

    2017, title The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations, MNRAS, 470, 4698, 10.1093/mnras/stx1517

    Anglés-Alcázar, D., Faucher-Giguère, C.-A., Kereš, D., et al. 2017, title The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations, MNRAS, 470, 4698, 10.1093/mnras/stx1517

    doi:10.1093/mnras/stx1517 2017

  8. [8]

    2004, title IAC - STAR : A Code for Synthetic Color - Magnitude Diagram Computation , AJ, 128, 1465, 10.1086/382836

    Aparicio, A., & Gallart, C. 2004, title IAC - STAR : A Code for Synthetic Color - Magnitude Diagram Computation , AJ, 128, 1465, 10.1086/382836

    work page doi:10.1086/382836 2004

  9. [9]

    2024, title Inflow and outflow properties, not total gas fractions, drive the evolution of the mass-metallicity relation, MNRAS, 532, L14, 10.1093/mnrasl/slae036

    Bassini, L., Feldmann, R., Gensior, J., et al. 2024, title Inflow and outflow properties, not total gas fractions, drive the evolution of the mass-metallicity relation, MNRAS, 532, L14, 10.1093/mnrasl/slae036

    doi:10.1093/mnrasl/slae036 2024

  10. [10]

    Benson, A. J. 2012, title Galacticus: A semi-analytic model of galaxy formation, New Astronomy, 17, 175, 10.1016/j.newast.2011.07.004

    doi:10.1016/j.newast.2011.07.004 2012

  11. [11]

    Benson, A. J. 2017, title The mass function of unprocessed dark matter haloes and merger tree branching rates, MNRAS, 467, 3454, 10.1093/mnras/stx343

    doi:10.1093/mnras/stx343 2017

  12. [12]

    J., Kamionkowski, M., & Hassani, S

    Benson, A. J., Kamionkowski, M., & Hassani, S. H. 2005, title Self-consistent theory of halo mergers, MNRAS, 357, 847, 10.1111/j.1365-2966.2005.08679.x

    arXiv 2005

  13. [13]

    J., Monelli, M., Gallart, C., et al

    Bernard, E. J., Monelli, M., Gallart, C., et al. 2013, title The ACS LCID Project - VIII. The short-period Cepheids of Leo A, MNRAS, 432, 3047, 10.1093/mnras/stt655

    work page doi:10.1093/mnras/stt655 2013

  14. [14]

    Z., Cannon, J

    Bernstein-Cooper, E. Z., Cannon, J. M., Elson, E. C., et al. 2014, title ALFALFA Discovery of the Nearby Gas-rich Dwarf Galaxy Leo P. V. Neutral Gas Dynamics and Kinematics, AJ, 148, 35, 10.1088/0004-6256/148/2/35

    doi:10.1088/0004-6256/148/2/35 2014

  15. [15]

    2021, title Distributions.jl: Definition and Modeling of Probability Distributions in the JuliaStats Ecosystem, Journal of Statistical Software, 98, 10.18637/jss.v098.i16

    Besançon, M., Papamarkou, T., Anthoff, D., et al. 2021, title Distributions.jl: Definition and Modeling of Probability Distributions in the JuliaStats Ecosystem, Journal of Statistical Software, 98, 10.18637/jss.v098.i16

    work page doi:10.18637/jss.v098.i16 2021

  16. [16]

    Bezanson, J., Edelman, A., Karpinski, S., & Shah, V. B. 2017, title Julia: A Fresh Approach to Numerical Computing, SIAM Review, 59, 65, 10.1137/141000671

    doi:10.1137/141000671 2017

  17. [17]

    O., Puls, J., & Najarro, F

    Bj \"o rklund, R., Sundqvist, J. O., Puls, J., & Najarro, F. 2021, title New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars. II. A grid of O-type stars in the Galaxy and the Magellanic Clouds, , 648, A36, 10.1051/0004-6361/202038384

    doi:10.1051/0004-6361/202038384 2021

  18. [18]

    A., Lu, Y., Benson, A., Katsianis, A., & Barraza, M

    Blanc, G. A., Lu, Y., Benson, A., Katsianis, A., & Barraza, M. 2019, title A Characteristic Mass Scale in the Mass - Metallicity Relation of Galaxies , ApJ, 877, 6, 10.3847/1538-4357/ab16ec

    doi:10.3847/1538-4357/ab16ec 2019

  19. [19]

    2006, title The Role of Pressure in GMC Formation II : The H2 - Pressure Relation , ApJ, 650, 933, 10.1086/505417

    Blitz, L., & Rosolowsky, E. 2006, title The Role of Pressure in GMC Formation II : The H2 - Pressure Relation , ApJ, 650, 933, 10.1086/505417

    doi:10.1086/505417 2006

  20. [20]

    R., Cole, S., Efstathiou, G., & Kaiser, N

    Bond, J. R., Cole, S., Efstathiou, G., & Kaiser, N. 1991, title Excursion set mass functions for hierarchical Gaussian fluctuations, ApJ, 379, 440, 10.1086/170520

    doi:10.1086/170520 1991

  21. [22]

    A., & Macci \`o , A

    Buck, T., Dutton, A. A., & Macci \`o , A. V. 2019, title An observational test for star formation prescriptions in cosmological hydrodynamical simulations, MNRAS, 486, 1481, 10.1093/mnras/stz969

    doi:10.1093/mnras/stz969 2019

  22. [23]

    Cappellari, M. 2023, title Full spectrum fitting with photometry in PPXF : stellar population versus dynamical masses, non-parametric star formation history and metallicity for 3200 LEGA - C galaxies at redshift z ≈ 0.8, MNRAS, 526, 3273, 10.1093/mnras/stad2597

    doi:10.1093/mnras/stad2597 2023

  23. [24]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, title The relationship between infrared, optical, and ultraviolet extinction , ApJ, 345, 245, 10.1086/167900

    doi:10.1086/167900 1989

  24. [25]

    Castelli, F., & Kurucz, R. L. 2003, in IAU Symposium, Vol. 210, Modelling of Stellar Atmospheres, ed. N. Piskunov , W. W. Weiss , & D. F. Gray , A20, 10.48550/arXiv.astro-ph/0405087

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0405087 2003

  25. [26]

    2003, title Galactic Stellar and Substellar Initial Mass Function, PASP, 115, 763, 10.1086/376392

    Chabrier, G. 2003, title Galactic Stellar and Substellar Initial Mass Function, PASP, 115, 763, 10.1086/376392

    doi:10.1086/376392 2003

  26. [27]

    2015, title PARSEC evolutionary tracks of massive stars up to 350 M ⊙ at metallicities 0.0001 ≤ Z ≤ 0.04, MNRAS, 452, 1068, 10.1093/mnras/stv1281

    Chen, Y., Bressan, A., Girardi, L., et al. 2015, title PARSEC evolutionary tracks of massive stars up to 350 M ⊙ at metallicities 0.0001 ≤ Z ≤ 0.04, MNRAS, 452, 1068, 10.1093/mnras/stv1281

    doi:10.1093/mnras/stv1281 2015

  27. [28]

    2014, title Improving PARSEC models for very low mass stars , MNRAS, 444, 2525, 10.1093/mnras/stu1605

    Chen, Y., Girardi, L., Bressan, a., et al. 2014, title Improving PARSEC models for very low mass stars , MNRAS, 444, 2525, 10.1093/mnras/stu1605

    doi:10.1093/mnras/stu1605 2014

  28. [29]

    2019, title YBC: a stellar bolometric corrections database with variable extinction coefficients

    Chen, Y., Girardi, L., Fu, X., et al. 2019, title YBC: a stellar bolometric corrections database with variable extinction coefficients. Application to PARSEC isochrones, , 632, A105, 10.1051/0004-6361/201936612

    doi:10.1051/0004-6361/201936612 2019

  29. [30]

    2018, title Metal-enriched galactic outflows shape the mass–metallicity relationship, MNRAS, 481, 1690, 10.1093/mnras/sty2380

    Chisholm, J., Tremonti, C., & Leitherer, C. 2018, title Metal-enriched galactic outflows shape the mass–metallicity relationship, MNRAS, 481, 1690, 10.1093/mnras/sty2380

    doi:10.1093/mnras/sty2380 2018

  30. [31]

    2016, title MESA ISOCHRONES AND STELLAR TRACKS ( MIST )

    Choi, J., Dotter, A., Conroy, C., et al. 2016, title MESA ISOCHRONES AND STELLAR TRACKS ( MIST ). I. SOLAR - SCALED MODELS , ApJ, 823, 102, 10.3847/0004-637x/823/2/102

    doi:10.3847/0004-637x/823/2/102 2016

  31. [32]

    R., Dav \'e , R., Governato, F., et al

    Christensen, C. R., Dav \'e , R., Governato, F., et al. 2016, title In-N-Out: The Gas Cycle from Dwarfs to Spiral Galaxies, ApJ, 824, 57, 10.3847/0004-637X/824/1/57

    doi:10.3847/0004-637x/824/1/57 2016

  32. [33]

    R., Davé, R., Brooks, A., Quinn, T., & Shen, S

    Christensen, C. R., Davé, R., Brooks, A., Quinn, T., & Shen, S. 2018, title Tracing Outflowing Metals in Simulations of Dwarf and Spiral Galaxies , ApJ, 867, 142, 10.3847/1538-4357/aae374

    doi:10.3847/1538-4357/aae374 2018

  33. [34]

    E., McQuinn, K

    Cohen, R. E., McQuinn, K. B. W., Savino, A., et al. 2025, title The JWST Resolved Stellar Populations Early Release Science Program . VIII . The Spatially Resolved Star Formation History of WLM , ApJ, 981, 153, 10.3847/1538-4357/adb61d

    doi:10.3847/1538-4357/adb61d 2025

  34. [35]

    A., Weisz, D

    Cole, A. A., Weisz, D. R., Dolphin, A. E., et al. 2014, title Delayed Star Formation in Isolated Dwarf galaxies: Hubble Space Telescope Star Formation History of the Aquarius Dwarf Irregular, ApJ, 795, 54, 10.1088/0004-637X/795/1/54

    doi:10.1088/0004-637x/795/1/54 2014

  35. [36]

    A., Skillman, E

    Cole, A. A., Skillman, E. D., Tolstoy, E., et al. 2007, title Leo A: A Late-blooming Survivor of the Epoch of Reionization in the Local Group, , 659, L17, 10.1086/516711

    doi:10.1086/516711 2007

  36. [37]

    J., Magdon-Ismail, M., et al

    Cole, N., Newberg, H. J., Magdon-Ismail, M., et al. 2008, title Maximum Likelihood Fitting of Tidal Streams with Application to the Sagittarius Dwarf Tidal Tails, ApJ, 683, 750, 10.1086/589681

    work page doi:10.1086/589681 2008

  37. [38]

    G., Baugh, C

    Cole, S., Lacey, C. G., Baugh, C. M., & Frenk, C. S. 2000, title Hierarchical galaxy formation, MNRAS, 319, 168, 10.1046/j.1365-8711.2000.03879.x

    arXiv 2000

  38. [39]

    2013, title Modeling the Panchromatic Spectral Energy Distributions of Galaxies, , 51, 393, 10.1146/annurev-astro-082812-141017

    Conroy, C. 2013, title Modeling the Panchromatic Spectral Energy Distributions of Galaxies, , 51, 393, 10.1146/annurev-astro-082812-141017

    doi:10.1146/annurev-astro-082812-141017 2013

  39. [40]

    G., & Lind, K

    Conroy, C., Villaume, A., van Dokkum, P. G., & Lind, K. 2018, title Metal-rich, Metal-poor: Updated Stellar Population Models for Old Stellar Systems, ApJ, 854, 139, 10.3847/1538-4357/aaab49

    doi:10.3847/1538-4357/aaab49 2018

  40. [41]

    2020, title The mass-metallicity and the fundamental metallicity relation revisited on a fully Te -based abundance scale for galaxies, MNRAS, 491, 944, 10.1093/mnras/stz2910

    Curti, M., Mannucci, F., Cresci, G., & Maiolino, R. 2020, title The mass-metallicity and the fundamental metallicity relation revisited on a fully Te -based abundance scale for galaxies, MNRAS, 491, 944, 10.1093/mnras/stz2910

    doi:10.1093/mnras/stz2910 2020

  41. [42]

    2024, title JADES: Insights into the low-mass end of the mass-metallicity-SFR relation at 3 < z < 10 from deep JWST/NIRSpec spectroscopy, , 684, A75, 10.1051/0004-6361/202346698

    Curti, M., Maiolino, R., Curtis-Lake, E., et al. 2024, title JADES: Insights into the low-mass end of the mass-metallicity-SFR relation at 3 < z < 10 from deep JWST/NIRSpec spectroscopy, , 684, A75, 10.1051/0004-6361/202346698

    doi:10.1051/0004-6361/202346698 2024

  42. [43]

    2019, title SIMBA: Cosmological simulations with black hole growth and feedback, MNRAS, 486, 2827, 10.1093/mnras/stz937

    Dav \'e , R., Angl \'e s-Alc \'a zar, D., Narayanan, D., et al. 2019, title SIMBA: Cosmological simulations with black hole growth and feedback, MNRAS, 486, 2827, 10.1093/mnras/stz937

    doi:10.1093/mnras/stz937 2019

  43. [44]

    Dav \'e , R., Finlator, K., & Oppenheimer, B. D. 2012, title An analytic model for the evolution of the stellar, gas and metal content of galaxies, MNRAS, 421, 98, 10.1111/j.1365-2966.2011.20148.x

    arXiv 2012

  44. [45]

    Davies, L. J. M., Robotham, A. S. G., del P Lagos, C., et al. 2019, title Galaxy And Mass Assembly ( GAMA ): Environmental Quenching of Centrals and Satellites in Groups, MNRAS, 483, 5444–5458, 10.1093/mnras/sty3393

    doi:10.1093/mnras/sty3393 2019

  45. [46]

    1997, title A new method to determine star formation histories of nearby galaxies, New Astronomy, 2, 397, 10.1016/S1384-1076(97)00029-8

    Dolphin, A. 1997, title A new method to determine star formation histories of nearby galaxies, New Astronomy, 2, 397, 10.1016/S1384-1076(97)00029-8

    work page doi:10.1016/s1384-1076(97)00029-8 1997

  46. [47]

    Dolphin, A. E. 2002, title Numerical methods of star formation history measurement and applications to seven dwarf spheroidals, MNRAS, 332, 91, 10.1046/j.1365-8711.2002.05271.x

    arXiv 2002

  47. [48]

    Dolphin, A. E. 2012, title On the Estimation of Systematic Uncertainties of Star Formation Histories, ApJ, 751, 60, 10.1088/0004-637x/751/1/60

    doi:10.1088/0004-637x/751/1/60 2012

  48. [49]

    Dolphin, A. E. 2016, title On the Incorporation of Metallicity Data Into Measurements of Star Formation History From Resolved Stellar Populations , ApJ, 825, 153, 10.3847/0004-637X/825/2/153

    work page doi:10.3847/0004-637x/825/2/153 2016

  49. [50]

    E., Saha, A., Skillman, E

    Dolphin, A. E., Saha, A., Skillman, E. D., et al. 2003, title Deep Hubble Space Telescope Imaging of Sextans A . III . The Star Formation History , AJ, 126, 187, 10.1086/375761

    doi:10.1086/375761 2003

  50. [51]

    2016, title MESA ISOCHRONES AND STELLAR TRACKS ( MIST ) 0: METHODS FOR THE CONSTRUCTION OF STELLAR ISOCHRONES , , 222, 8, 10.3847/0067-0049/222/1/8

    Dotter, A. 2016, title MESA ISOCHRONES AND STELLAR TRACKS ( MIST ) 0: METHODS FOR THE CONSTRUCTION OF STELLAR ISOCHRONES , , 222, 8, 10.3847/0067-0049/222/1/8

    doi:10.3847/0067-0049/222/1/8 2016

  51. [52]

    The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies

    Durbin, M. J., Choi, Y., Savino, A., et al. 2025, title The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies, ArXiv e-prints, arXiv:2505.18252, 10.48550/arXiv.2505.18252

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2505.18252 2025

  52. [53]

    L., & Mac Low, M.-M

    Emerick, A., Bryan, G. L., & Mac Low, M.-M. 2018, title Stellar Radiation Is Critical for Regulating Star Formation and Driving Outflows in Low-mass Dwarf Galaxies, ApJL, 865, L22, 10.3847/2041-8213/aae315

    doi:10.3847/2041-8213/aae315 2018

  53. [54]

    N., et al

    Escala, I., Wetzel, A., Kirby, E. N., et al. 2018, title Modelling chemical abundance distributions for dwarf galaxies in the Local Group : the impact of turbulent metal diffusion, MNRAS, 474, 2194, 10.1093/mnras/stx2858

    doi:10.1093/mnras/stx2858 2018

  54. [55]

    J., Castro, N., Gonzalez, O

    Evans, C. J., Castro, N., Gonzalez, O. A., et al. 2019, title First stellar spectroscopy in Leo P, A & A, 622, A129, 10.1051/0004-6361/201834145

    work page doi:10.1051/0004-6361/201834145 2019

  55. [56]

    2015, title The equilibrium view on dust and metals in galaxies: Galactic outflows drive low dust-to-metal ratios in dwarf galaxies, MNRAS, 449, 3274, 10.1093/mnras/stv552

    Feldmann, R. 2015, title The equilibrium view on dust and metals in galaxies: Galactic outflows drive low dust-to-metal ratios in dwarf galaxies, MNRAS, 449, 3274, 10.1093/mnras/stv552

    doi:10.1093/mnras/stv552 2015

  56. [57]

    2023, title FIREbox : simulating galaxies at high dynamic range in a cosmological volume, MNRAS, 522, 3831, 10.1093/mnras/stad1205

    Feldmann, R., Quataert, E., Faucher-Giguère, C.-A., et al. 2023, title FIREbox : simulating galaxies at high dynamic range in a cosmological volume, MNRAS, 522, 3831, 10.1093/mnras/stad1205

    doi:10.1093/mnras/stad1205 2023

  57. [58]

    Gallart, C., Zoccali, M., & Aparicio, A. 2005, title The Adequacy of Stellar Evolution Models for the Interpretation of the Color - Magnitude Diagrams of Resolved Stellar Populations , , 43, 387, 10.1146/annurev.astro.43.072103.150608

    Pith/arXiv arXiv 2005

  58. [59]

    M., Torrey, P., Grasha, K., et al

    Garcia, A. M., Torrey, P., Grasha, K., et al. 2024 a , title Interplay of stellar and gas-phase metallicities: unveiling insights for stellar feedback modelling with Illustris, IllustrisTNG, and EAGLE, MNRAS, 529, 3342, 10.1093/mnras/stae737

    doi:10.1093/mnras/stae737 2024

  59. [60]

    M., Torrey, P., Ellison, S., et al

    Garcia, A. M., Torrey, P., Ellison, S., et al. 2024 b , title Does the fundamental metallicity relation evolve with redshift? I : the correlation between offsets from the mass-metallicity relation and star formation rate, MNRAS, 531, 1398, 10.1093/mnras/stae1252

    doi:10.1093/mnras/stae1252 2024

  60. [61]

    M., Torrey, P., Bhagwat, A., et al

    Garcia, A. M., Torrey, P., Bhagwat, A., et al. 2025 a , title Metallicity Gradients in Modern Cosmological Simulations I : Tension Between Smooth Stellar Feedback Models and Observations , ApJ, 989, 147, 10.3847/1538-4357/adea51

    doi:10.3847/1538-4357/adea51 2025

  61. [62]

    M., Torrey, P., Ellison, S

    Garcia, A. M., Torrey, P., Ellison, S. L., et al. 2025 b , title Does the fundamental metallicity relation evolve with redshift? - II . The evolution in normalization of the mass-metallicity relation, MNRAS, 536, 119, 10.1093/mnras/stae2587

    doi:10.1093/mnras/stae2587 2025

  62. [63]

    2025, title StarFormationHistories.jl, Zenodo, 10.5281/zenodo.14963317

    Garling, C. 2025, title StarFormationHistories.jl, Zenodo, 10.5281/zenodo.14963317

    work page doi:10.5281/zenodo.14963317 2025

  63. [64]

    T., Kallivayalil, N., McQuinn, K

    Garling, C. T., Kallivayalil, N., McQuinn, K. B. W., et al. 2025, title Measuring Resolved Star Formation Histories from High - Precision Color - Magnitude Diagrams with StarFormationHistories .jl, ApJS, 277, 25, 10.3847/1538-4365/adbb64

    work page doi:10.3847/1538-4365/adbb64 2025

  64. [65]

    Gill, S. P. D., Knebe, A., & Gibson, B. K. 2004, title The evolution of substructure - I. A new identification method, MNRAS, 351, 399, 10.1111/j.1365-2966.2004.07786.x

    arXiv 2004

  65. [66]

    P., Adams, E

    Giovanelli, R., Haynes, M. P., Adams, E. A. K., et al. 2013, title ALFALFA Discovery of the Nearby Gas-rich Dwarf Galaxy Leo P. I. H I Observations, , 146, 15, 10.1088/0004-6256/146/1/15

    doi:10.1088/0004-6256/146/1/15 2013

  66. [67]

    D., Fouesneau, M., Arab, H., et al

    Gordon, K. D., Fouesneau, M., Arab, H., et al. 2016, title The Panchromatic Hubble Andromeda Treasury. XV. The BEAST: Bayesian Extinction and Stellar Tool, , 826, 104, 10.3847/0004-637X/826/2/104

    doi:10.3847/0004-637x/826/2/104 2016

  67. [68]

    M., van Hoof, P

    Gunasekera, C. M., van Hoof, P. A. M., Chatzikos, M., & Ferland, G. J. 2023, title The 23.01 Release of Cloudy , RNAAS, 7, 246, 10.3847/2515-5172/ad0e75

    doi:10.3847/2515-5172/ad0e75 2023

  68. [69]

    2019, title The origins of the circumgalactic medium in the FIRE simulations, MNRAS, 488, 1248, 10.1093/mnras/stz1773

    Hafen, Z., Faucher-Gigu \` e re, C.-A., Angl \' e s-Alc \' a zar, D., et al. 2019, title The origins of the circumgalactic medium in the FIRE simulations, MNRAS, 488, 1248, 10.1093/mnras/stz1773

    doi:10.1093/mnras/stz1773 2019

  69. [70]

    J., Adams, N

    Harvey, T., Conselice, C. J., Adams, N. J., et al. 2025, title Behind the spotlight: a systematic assessment of outshining using NIRCam medium bands in the JADES Origins Field, MNRAS, 542, 2998, 10.1093/mnras/staf1396

    doi:10.1093/mnras/staf1396 2025

  70. [71]

    2024, title Empirical mass-loss rates and clumping properties of O-type stars in the Large Magellanic Cloud, , 690, A126, 10.1051/0004-6361/202348478

    Hawcroft, C., Mahy, L., Sana, H., et al. 2024, title Empirical mass-loss rates and clumping properties of O-type stars in the Large Magellanic Cloud, , 690, A126, 10.1051/0004-6361/202348478

    doi:10.1051/0004-6361/202348478 2024

  71. [72]

    2020, title Kinematic and metallicity properties of the Aquarius dwarf galaxy from FORS2 MXU spectroscopy, , 634, A10, 10.1051/0004-6361/201936136

    Hermosa Mu \ n oz, L., Taibi, S., Battaglia, G., et al. 2020, title Kinematic and metallicity properties of the Aquarius dwarf galaxy from FORS2 MXU spectroscopy, , 634, A10, 10.1051/0004-6361/201936136

    work page doi:10.1051/0004-6361/201936136 2020

  72. [73]

    L., Pietrinferni, A., Cassisi, S., et al

    Hidalgo, S. L., Pietrinferni, A., Cassisi, S., et al. 2018, title The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations, ApJ, 856, 125, 10.3847/1538-4357/aab158

    doi:10.3847/1538-4357/aab158 2018

  73. [74]

    F., Kere s , D., O \ n orbe, J., et al

    Hopkins, P. F., Kere s , D., O \ n orbe, J., et al. 2014, title Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation, MNRAS, 445, 581, 10.1093/mnras/stu1738

    doi:10.1093/mnras/stu1738 2014

  74. [75]

    F., Wetzel, A., Kere s , D., et al

    Hopkins, P. F., Wetzel, A., Kere s , D., et al. 2018, title FIRE-2 simulations: physics versus numerics in galaxy formation, MNRAS, 480, 800, 10.1093/mnras/sty1690

    doi:10.1093/mnras/sty1690 2018

  75. [76]

    F., Wetzel, A., Wheeler, C., et al

    Hopkins, P. F., Wetzel, A., Wheeler, C., et al. 2023, title FIRE -3: updated stellar evolution models, yields, and microphysics and fitting functions for applications in galaxy simulations, MNRAS, 519, 3154, 10.1093/mnras/stac3489

    doi:10.1093/mnras/stac3489 2023

  76. [77]

    A., Ficut-Vicas, D., Ashley, T., et al

    Hunter, D. A., Ficut-Vicas, D., Ashley, T., et al. 2012, title Little Things, AJ, 144, 134, 10.1088/0004-6256/144/5/134

    doi:10.1088/0004-6256/144/5/134 2012

  77. [78]

    Hunter, J. D. 2007, title Matplotlib: A 2D graphics environment, Computing In Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    doi:10.1109/mcse.2007.55 2007

  78. [79]

    Ianjamasimanana, R., Namumba, B., Ramaila, A. J. T., et al. 2020, title MeerKAT -16 H I observation of the dIrr galaxy WLM , MNRAS, 497, 4795, 10.1093/mnras/staa1967

    doi:10.1093/mnras/staa1967 2020

  79. [80]

    L., Khostovan, A

    Jain, S., Sanders, R. L., Khostovan, A. A., et al. 2025, title A Uniform Analysis of Gas-phase Metallicity Evolution with 1-3 Gyr Time Sampling over the Past 12 Billion Years, ArXiv e-prints, 10.48550/ARXIV.2508.18369

    Pith/arXiv arXiv doi:10.48550/arxiv.2508.18369 2025

  80. [81]

    Jiang, F., & van den Bosch, F. C. 2014, title Generating merger trees for dark matter haloes: a comparison of methods, MNRAS, 440, 193, 10.1093/mnras/stu280

    doi:10.1093/mnras/stu280 2014

Showing first 80 references.

This paper was first reviewed by deepseek-v4-flash on August 4, 2026.